arXiv subjects

S. B. Shaulov

Publications and source records attributed to S. B. Shaulov.

6 recordsLinked to original sources

arXiv2022

The composition of cosmic rays according to the data on EAS cores

The main purpose of this work is to find the causes of the break of the cosmic ray spectrum at an energy of 3 PeV, which is called the knee. The solution of the problem is associated with the determination of the nuclear composition of cosmic rays in the knee area. The conclusions of this work are based on the analysis of the characteristics of the EAS cores obtained using X-ray emulsion chambers. According to these data, a number of anomalous effects are observed in the knee region, such as scaling violation in the spectra of secondary hadrons, an excess of muons in EAS with gamma families and others. At the same energies equivalent to 1-100 PeV the laboratory system colliders show scaling behavior. So analysis of the data on the EAS cores suggests that the knee in their spectrum is formed by a component of cosmic rays of a non-nuclear nature, possibly consisting of stable (quasi-stable) particles of hypothetical strange quark matter, which named strangelets. This is the only model of the knee compatible with the magnetic rigidity of the nuclear spectra break R=100 TV. In fact, stranglets are stable heavy quasi-nuclei with a positive electric charge of Z=30-1000, so the mechanism of their acceleration coincides with the nuclear one. The break of the cosmic ray spectrum can be associated with a significantly larger mass of strangelets compared to nuclei.

astro-ph.HE↗

arXiv2019

New complex EAS installation of the Tien Shan Mountain Cosmic Ray Station

We present a description of the new complex installation for the study of extensive air showers which was created at the Tien Shan mountain cosmic ray station, as well as the results of the test measurements made there in 2014-2016. At present, the system for registration of electromagnetic shower component consists of $\sim$100 detector points built on the basis of plastic scintillator plates with the sensitive area of 0.25m$^2$ and 1m$^2$, spread equidistantly over $\sim$10$^4$m$^2$ space. The dynamic range of scintillation amplitude measurements is currently about $(3-7)\cdot 10^4$, and there is a prospect of it being extended up to $\sim$10$^6$. The direction of shower arrival is defined by signal delays from a number of the scintillators placed cross-wise at the periphery of the detector system. For the investigation of nuclear active shower components there was created a multi-tier 55m$^2$ ionization-neutron calorimeter with a sum absorber thickness of $\sim$1000g/cm$^2$, typical spatial resolution of the order of 10cm, and dynamic range of ionization measurement channel about $\sim$10$^5$. Also, the use of saturation-free neutron detectors is anticipated for registration of the high- and low-energy hadron components in the region of shower core. A complex of underground detectors is designed for the study of muonic and penetrative nuclear-active components of the shower. The full stack of data acquisition, detector calibration, and shower parameters restoration procedures are now completed, and the newly obtained shower size spectrum and lateral distribution of shower particles occur in agreement with conventional data. Future studies in the field of $10^{14}-10^{17}$eV cosmic ray physics to be held at the new shower installation are discussed.

astro-ph.HE↗

arXiv2019

EAS data at the mountain level and a shape of the CR spectrum beyond the break

In the most works which deal with EAS the CR energy spectrum is deduced by means of the model defined dependence $E_0=a\cdot{N_e}^α$. An electron total number $N_e$ is evaluated by integration of the NKG-function f(r). This algorithm breaks down for young EAS with age parameter $s\sim0$. This work shows, that part of the young EAS becomes large in the range $N_e\geq10^7$, it cause to divergency of the $N_e$ integral for them and distorts the shape of EAS (CR) spectrum. A final analysis of the experimental data permits to conclude that EAS spectrum has local maximum at $N_e\sim10^9$, which results in a decrease of the EAS spectrum slope for $N_e\geq10^7$ (inverse break or "knee"). A local maximum can arise because of the additional CR component in the range $E_0\geq10$ PeV.

astro-ph.HE↗

arXiv2018

gamma-Families with Halos Observed by X-ray Emulsion Chamber in EAS and the Estimate of the p+He Fraction in Primary Cosmic Rays at E0 = 1-100 PeV

The experimental gamma-families in which events called "halos" were detected using X-ray emulsion chambers (XRECs) of the PAMIR experiment are described. The halo nature is explained within the standard model of nuclear interactions. Based on events with halo, the fraction of p+He in primary cosmic rays (PCR) was estimated. It is shown that the PCR mass composition remains mixed in the range E0 = 1-100 PeV.

astro-ph.HE↗

arXiv2012

Results on the primary CR spectrum and composition reconstructed with the SPHERE-2 detector

First preliminary results of the balloon-borne experiment SPHERE-2 on the all-nuclei primary cosmic rays (PCR) spectrum and primary composition are presented. The primary spectrum in the energy range $10^{16}$--$5\cdot10^{17}$ eV was reconstructed using characteristics of Vavilov-Cherenkov radiation of extensive air showers (EAS), reflected from a snow surface. Several sources of systematic uncertainties of the spectrum were analysed. A method for separation of the primary nuclei' groups based on the lateral distribution function' (LDF) steepness parameter is presented. Preliminary estimate of the mean light nuclei' fraction $f_{30-150}$ at energies $3\cdot10^{16}$--$1.5\cdot10^{17}$ eV was performed and yielded $f_{30-150}$= (21$\pm$11)%.

astro-ph.HE↗

arXiv2012

Status of the SPHERE experiment

Here is presented the current state of the SPHERE-2 balloon-borne experiment. The detector is elevated up to 1 km above the snow surface and registers the reflected Vavilov-Cherenkov radiation from extensive air showers. This method has good sensitivity to the mass-composition of the primary cosmic rays due to its high resolution near the shower axis. The detector consists of a 1500 mm spherical mirror with a 109 PMT cluster in its focus. The electronics record a signal pulse profile in each PMT. In the last 2 years the detector was upgraded: time resolution of pulse registration was enhanced up to 12.5 ns, channel sensitivity was increased by a factor of 3, a new LED-based relative PMT calibration method was introduced, and new hardware and etc. was installed.

astro-ph.IM↗